**Part 4**

**The Solar Wind Magnetic Field Powered by the Sun** 

18 Exploring the Solar Wind

258 Exploring the Solar Wind

Pierrard V. & Lamy H. (2003). The effects of the velocity filtration mechanism on the minor

Pilipp W.G., Miggenrieder H., Montgomery M.D., et al. (1987). Variations of electron

Prested C., Schwadron N., Passuite J, et al. (2008). Implications of solar wind suprathermal tails for IBEX ENA images of the heliosheath, *J. Geophys. Res.* 113, A06102. Roberts D.A. & Miller J.A. (1998). Generation of nonthermal electron distributions by

Saito S. & Gary S.P. (2007). Whistler scattering of suprathermal electrons in the solar wind:

Scudder J.D. (1992). On the causes of temperature change in inhomogenous low-density

Stverak, S.; Travnicek, P.; Maksimovic, M. et al. (2008). Electron temperature anisotropy

Summers D. & Ma C. (2000). Rapid acceleration of electrons in the magnetosphere by

Treumann R.A. & Jaroschek C.H. (2008). Gibbsian theory of power-law distributions, *Phys.*

Tsallis C. (1995). Non-extensive thermostatistics: brief review and comments, *Phys. A*, 221,

Tylka A.J., Cohen C.M.S., Dietrich W.F., et al. (2001). Evidence for remnant flare suprathermals

Vasyliunas V.M. (1968). A Survey of low-energy electrons in the evening sector of the

Viñas A.F., Wong H.K. & Klimas A.J. (2000). Generation of electron suprathermal tails in the upper solar atmosphere: implications for coronal heating, *Astrophys. J.* 528, 509. Viñas A.F., Mace R.L. & Benson RF. (2005). Dispersion characteristics for plasma resonances

Vocks C. & Mann G. (2003). Generation of suprathermal electrons by resonant wave-particle

Vocks C., Salem C., Lin R.P. & Mann G. (2005). Electron halo and strahl formation in the solar wind by resonant interaction with whistler waves, *Astroph. J.* 627, 540. Yoon P.H., T. Rhee & C.-M. Ryu (2006). Self-consistent formation of electron *κ* distribution: 1.

Zouganelis I., Maksimovic M., Meyer-Vernet N., et al. (2004). A transonic collisionless model

Zouganelis I. (2008). Measuring suprathermal electron parameters in space plasmas:

Implementation of the quasi-thermal noise spectroscopy with kappa distributions using in situ Ulysses/URAP radio measurements in the solar wind, *J. Geophys. Res.*

magnetosphere with OGO 1 and OGO 3, *J. Geophys. Res.* 73, 2839.

IMAGE/RPI observations, *J. Geophys. Res.* 110, A06202.

Theory, *J. Geophys. Res.* 111, A09106.

of the solar wind, *Astrophys. J.* 606, 542.

interaction in the solar corona and wind, *Astroph. J.* 593, 1134.

in the source population of solar energetic particles in the 2000 Bastille Day event,

of Maxwellian and Kappa distribution plasmas and their comparisons to the

distribution functions in the solar wind, *J. Geophys. Res.* 92, 1075.

turbulent waves near the Sun, *Geophys. Res. Lett.* 25, 607.

Particle-in-cell simulations, *J. Geophys. Res.*, 112, A06116. Schlickeiser R. (2002). *Cosmic Ray Astrophysics*, Springer, Heidelberg.

constraints in the solar wind, *J. Geophys. Res.*, 113, A03103.

fast-mode MHD waves, *J. Geophys. Res.* 105, 15,887.

astrophysical plasmas, *Astrophys. J.* 398, 299.

*Rev. Lett.* 100, 155005.

*Astrophys. J.* 558, L59.

113, A08111.

277.

ions of the corona, *Solar Phys.* 216, 47.

**12** 

*Russia* 

**Impact of the Large-Scale Solar Magnetic Field** 

In 1955 Soviet astrophysicists Vsehsvyatskiy, Nikolskiy, Ponomarev and Cherednichenko (Vsekhsvyatskiy et al., 1955) showed that broad corona loses its energy for radiance, and can be in hydrodynamic equilibrium, and there should be a flow of materials and energy.

This process is a physical basis for the important phenomenon of "dynamic corona". The magnitude of the flow of materials was evaluated due to the following considerations: if the corona were in hydrodynamic equilibrium, then the altitudes of homogenous atmosphere for hydrogen and iron would correlate as 56/1. In other words, in such case iron ions must not be observed in the distant corona. But this is not so. In 1955 it was a considerable

Three years later Eugene N. Parker came to the conclusion that hot solar stream in Chapman model and particle flux, blowing away commentary tails in Birmann's hypothesis – these are manifestation of the same phenomenon, and Eugene N. Parker called it "solar wind".

Parker (Parker, 1958) showed - despite the fact that solar corona is greatly gravitated to the Sun, it is a strong heat conductor, it remains hot even at great distance. The farther the distance, the less the solar gravitation is, there is a supersonic discharge from the upper

Solar wind represents a flux of ionized particles, thrown out of the Sun in all the directions with the speed about 300-1200 km/sec. The source of the solar wind is solar corona. The temperature of the solar corona is so high, that gravitation force is not able to hold its substance near the surface, and part of this substance constantly moves to interplanetary

First direct gaging of the solar wind was carried out in 1959 by the automatic interplanetary station "Luna-1". The observations were made by means of a scintillometer and a gas ionization detector. Three years later the same gaging was implemented by the American

achievement, but nobody believed in the phenomenon of "dynamic corona".

**1. Introduction** 

corona into interplanetary space.

scientists on board the station "Mariner-2".

space.

**on the Solar Corona and Solar Wind** 

*Russian Academy of Sciences, Troitsk, Moscow Region* 

A.G. Tlatov1 and B.P. Filippov2 *1Kislovodsk Mountain Station of the Central Astronomical Observatory of RAS at Pulkovo 2Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation,* 
